0Assigned ID: 1929
----- Attempting Submission 1 (Fri Mar 01 23:20:33 GMT 2013) -----Comments about personel and software:
I found APT a fantastically useful program for preparing Phase II.
I thought Paule Sonnentrucker was extremely helpful and knowledgable about the whole process.
Software suggestion/comment:
One aspect of APT (perhaps a bug?) that became slightly annoying was when editing the buffer times. To reproduce the bug, if you enter a number, say 107534, then move your cursor to the left most part of the text box, and then press the right arrow key, some of the numbers are deleted. Perhaps this is so the buffer time doesn't exceed the exposure time (probably a good idea)? A similar problem happens if you're at the rightmost character and you move left one place, the rightmost character tends to be highlighted. If you now enter a number it will write over the rightmost character which isn't desirable.
Thanks very much,
Ryan.-152317447----- Attempting Submission 1 (Sat Jun 22 05:53:06 GMT 2013) -----Several warnings remain in this proposal. There are 4 "Visit Overun" warnings, which are not a problem since the observations are deemed schedulable with the visit planner, and it's just 1s or 2s in these 4 cases. There are also 2 bright object warnings from the GSCII catalog. This is because the BOT has assumed that my targets are unreddened O5 V stars while my science targets are QSOs. The ETC calculations (ETC ID numbers are provided) have shown that these targets are safe. As a result the BOT warning is not appropriate to my proposal and can be safely ignored.Primordial lithium in z~0, metal-poor damped Lyman alpha systemsA longstanding challenge for the standard model of Big Bang Nucleosynthesis is to explain the discrepancy between the predicted and observed primordial lithium abundance; the most metal-poor stars are deficient in Li by a factor of 3-4 relative to the standard model prediction. We propose to use the combined efforts of HST+COS and ground-based optical echelle spectrographs, to measure the primordial Li abundance in clouds of near-pristine gas at low redshift. To this end, we have compiled a prime list of sure candidate low-redshift damped Lyman-alpha systems (DLAs) that are in front of bright quasars. This combination is essential to detect the weak Li absorption lines arising in the ISM of external galaxies. For a small investment of HST time, we will confirm these systems as new low-redshift DLAs -- almost tripling the current number of known systems -- and discern the optimum clouds where the primordial abundance of Li can be measured. The sought-after data will also provide new opportunities to study the detailed properties of DLAs and their host galaxies, as well as the greater environments in which they reside.Summary: The main goal of our HST+COS program is to discover damped Lyman-alpha systems (DLAs) at low redshift (z_abs < 0.3) and in front of bright quasars. The two primary objectives are to: (1) Find metal-poor DLAs where we can measure the primordial abundance of Li; and (2) understand the properties of low-redshift DLAs.
Targets and Acquisition: We will target 9 quasars total, with FUV magnitudes in the range 16.7-17.8, which intersect 11 candidate DLAs. Since our target coordinates are precisely known from SDSS, we will acquire our targets with the ACQ/IMAGE acquisition mode. Using the GALEX FUV magnitudes of our targets, we have calculated the exposure times that are required to achieve the recommended S/N of 40 (ETC ID numbers are provided). We have increased these exposure times by 20 per cent to account for QSO variability.
Science Exposures: We will observe in TIME-TAG mode, and use the standard wavelength calibration procedures (i.e. with TAGFLASH=YES). We will observe each system at all four FP-POS settings (obtained in increasing order). We have performed an ETC calculation for each grating setup (ETC ID numbers are provided). We opted to dump the buffer 100s before the end of each science exposure to minimize the TIME-TAG memory read-out times between exposures. To achieve our science goals, we only require a final combined S/N ~ 10 at certain wavelengths, which will be satisfied for most targets with just one orbit.
Bright-Object Protection: Both local and global limits are confirmed as safe for the target fields to be observed. Our targets are several magnitudes fainter than the unsafe limits. We expect that the brightest feature in our spectrum will be the geocoronal Lyman-alpha airglow emission line.QUASAR ABSORPTION LINES AND IGMDefaultfalsetruefalsefalsefalseSUPPORTEDEXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICDAMPED LYMAN ALPHA CLOUDJ2000FUV magnitude=17.75EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICDAMPED LYMAN ALPHA CLOUDJ2000J2000FUV magnitude=17.11EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICDAMPED LYMAN ALPHA CLOUDJ2000FUV magnitude=17.83EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICDAMPED LYMAN ALPHA CLOUDJ2000J2000FUV magnitude=17.56EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICDAMPED LYMAN ALPHA CLOUDJ2000FUV magnitude=17.23EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICDAMPED LYMAN ALPHA CLOUDJ2000FUV magnitude=17.47EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICDAMPED LYMAN ALPHA CLOUDJ2000J2000FUV magnitude=17.41EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICDAMPED LYMAN ALPHA CLOUDJ2000FUV magnitude=16.90EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICDAMPED LYMAN ALPHA CLOUDJ2000J2000FUV magnitude=16.71COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1327/private/var/folders/2x/5q455gl14rq1mbr5sj63x6_80000gn/T/OPVisit2791185574186922891.xmlThe scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.(Tic-Visit
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